标题： 行星-涡旋相互作用：涡旋如何引导行星胚胎 显示英文标题

标题： Planet-vortex interaction:How a vortex can shepherd a planetary embryo

摘要： 背景：反气旋涡被认为是有利的尘埃聚集地和行星胚胎形成的场所。 另一方面，它们是巨大的团块，可以与盘中的行星产生引力相互作用。 目的：我们旨在研究涡旋如何以引力方式与向其迁移的行星或在涡旋内部形成的行星相互作用。 方法：我们使用GFARGO和FARGO-ADSG进行了粘性局部等温盘的流体力学模拟。 我们以一种方式在盘中设置了一个稳定的高斯压力隆起，从而触发了RWI（Rossby波不稳定性）。 在大涡旋形成后，我们在外部盘或涡旋内部植入了一个低质量行星，并允许其迁移。 我们还检查了涡旋强度对行星迁移的影响，并在存在自引力的情况下验证了最终结果的有效性。 结果：我们注意到，无论行星的初始位置如何，最终行星都会被锁定到涡旋上，或者在更强的涡旋情况下，在更远的轨道距离处停止迁移。 对于较弱涡旋的模型，我们研究了不同参数的影响，包括背景粘度、背景表面密度、行星质量和不同的行星位置。 在这些模型中，尽管行星捕获时间和锁定角度因不同参数而变化，但主要结果——行星-涡旋锁定——仍然有效。 我们发现，即使质量小于5×10^{-7} M_{\star }的行星也能从涡旋中出来并在相同的轨道距离处被锁定。 对于较强的涡旋，无论是非自引力还是自引力模型，行星的迁移都在远离涡旋径向位置的地方停止。 这种效应可以使涡旋在行星增长过程中保持形状的条件下成为持续行星形成的合适场所。 显示英文摘要

摘要： Context: Anticyclonic vortices are considered as a favourable places for trapping dust and forming planetary embryos. On the other hand, they are massive blobs that can interact gravitationally with the planets in the disc. Aims: We aim to study how a vortex interacts gravitationally with a planet which migrates toward it or a planet which is created inside the vortex. Methods: We performed hydrodynamical simulations of a viscous locally isothermal disc using GFARGO and FARGO-ADSG. We set a stationary Gaussian pressure bump in the disc in a way that RWI is triggered. After a large vortex is established, we implanted a low mass planet in the outer disc or inside the vortex and allowed it to migrate. We also examined the effect of vortex strength on the planet migration and checked the validity of the final result in the presence of self-gravity. Results: We noticed regardless of the planet's initial position, the planet is finally locked to the vortex or its migration is stopped in a farther orbital distance in case of a stronger vortex. For the model with the weaker vortex, we studied the effect of different parameters such as background viscosity, background surface density, mass of the planet and different planet positions. In these models, while the trapping time and locking angle of the planet vary for different parameters, the main result, which is the planet-vortex locking, remains valid. We discovered that even a planet with a mass less than 5 * 10^{-7} M_{\star} comes out from the vortex and is locked to it at the same orbital distance. For a stronger vortex, both in non-self-gravitated and self-gravitating models, the planet migration is stopped far away from the radial position of the vortex. This effect can make the vortices a suitable place for continual planet formation under the condition that they save their shape during the planetary growth.